HD 104067 is a star with a planetary system in the southern constellation of Corvus. It has an apparent visual magnitude of 7.92[2] which is too faint to be visible with the naked eye. The distance to this star is 66.4 light-years (20.4 parsecs) based on parallax. It is drifting further away with a radial velocity of +15 km/s.[1]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Corvus |
| Right ascension | 11h 59m 10.00884s[1] |
| Declination | −20° 21′ 13.6121″[1] |
| Apparent magnitude (V) | 7.92[2] |
| Characteristics | |
| Spectral type | K3V[3] |
| Apparent magnitude (B) | 8.894[2] |
| Apparent magnitude (J) | 6.212±0.019[2] |
| Apparent magnitude (H) | 5.754±0.023[2] |
| Apparent magnitude (K) | 5.614±0.024[2] |
| B−V color index | 0.974±0.010[2] |
| Astrometry | |
| Radial velocity (Rv) | +14.89±0.12[1] km/s |
| Proper motion (μ) | RA: 141.706 mas/yr[1] Dec.: −423.780 mas/yr[1] |
| Parallax (π) | 49.1470 ± 0.0235 mas[1] |
| Distance | 66.36 ± 0.03 ly (20.347 ± 0.010 pc) |
| Absolute magnitude (MV) | 6.30[2] |
| Details | |
| Mass | 0.818+0.024 −0.025[4] M☉ |
| Radius | 0.771+0.007 −0.006[4] R☉ |
| Luminosity | 0.307[5] L☉ |
| Surface gravity (log g) | 4.56±0.10[6] cgs |
| Temperature | 4,942±14[4] K |
| Metallicity [Fe/H] | 0.11±0.06[6] dex |
| Rotation | 18.3±4.9 d[6] |
| Rotational velocity (v sin i) | 2.47±0.96[4] km/s |
| Age | 4.8+3.3 −3.0[4] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
This is an ordinary K-type main-sequence star with a stellar classification of K3V.[3] It is a moderately active star[8] with an age of roughly five billion years. HD 104067 is spinning with a projected rotational velocity of 2.5 km/s,[4] giving it a rotation period of approximately a month.[3] The star has 82% of the mass and 77% of the radius of the Sun.[4] It is radiating 31%[5] of the Sun's luminosity from its photosphere at an effective temperature of 4,942 K. The metal content of this star is close to that in the Sun.[4]
Planetary system
editHD 104067 has been observed as part of the HARPS planet-finding survey since 2004. The detection of an exoplanetary companion using the radial velocity method was announced in 2011. This sub-Saturn planet, HD 104067 b, has at least 0.2 times the mass of Jupiter and takes 55.8 days to orbit the star at a distance of 0.26 AU.[8] The discovery of a second, Uranus-mass planet, HD 104067 c, was announced in 2024 based on HARPS and HIRES data. TESS observations also show evidence of a third candidate planet, slightly larger than Earth and orbiting closer to the star than the other two planets, with a period of just 2.2 days. Modeling suggests that this inner planet candidate may experience significant tidal heating.[6]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| TOI-6713.01 (unconfirmed) | — | 0.03054(37) | 2.1538197(41) | — | 86.5±2.0° | 1.30±0.12 R🜨 |
| c | ≥13.2±1.9 M🜨 | 0.1058±0.0013 | 13.8992+0.0047 −0.0037 |
0.29+0.12 −0.13 |
— | — |
| b | ≥62.1+3.3 −3.2 M🜨 |
0.2674+0.0032 −0.0033 |
55.851±0.017 | 0.123+0.048 −0.051 |
— | — |
See also
editReferences
edit- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f g h Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
- ^ a b c Suárez Mascareño, A.; et al. (September 2015). "Rotation periods of late-type dwarf stars from time series high-resolution spectroscopy of chromospheric indicators". Monthly Notices of the Royal Astronomical Society. 452 (3): 2745–2756. arXiv:1506.08039. Bibcode:2015MNRAS.452.2745S. doi:10.1093/mnras/stv1441. S2CID 119181646.
- ^ a b c d e f g h Soto, M. G.; Jenkins, J. S. (2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy and Astrophysics. 615: A76. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. S2CID 119107228.
- ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e Kane, Stephen R.; Fetherolf, Tara; et al. (March 2024). "A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World". The Astronomical Journal. 167 (5): 239. arXiv:2403.17062. Bibcode:2024AJ....167..239K. doi:10.3847/1538-3881/ad3820.
- ^ "HD 104067". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2021-09-28.
- ^ a b Ségransan, D.; et al. (2011). "The HARPS search for southern extra-solar planets. XXIX. Four new planets in orbit around the moderately active dwarfs HD 63765, HD 104067, HD 125595, and HIP 70849". Astronomy and Astrophysics. 535. A54. arXiv:1107.0339. Bibcode:2011A&A...535A..54S. doi:10.1051/0004-6361/200913580. S2CID 119197766.